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Rotational Mixing in Massive Stars Kim Venn Abstract Rotation is now recognized as an important physical component in understanding massive star evolution. Theory suggests that rotation affects the lifetimes, chemical yields, stellar evolution tracks, and the supernova and compact remnant properties (Heger & Langer 2000, Maeder & Meynet 2000). In a series of HST programs, we have been exploiting the B III 2066 A resonance line in main sequence B-stars to test the efficiency of rotational mixing. We have proved that rotational mixing must occur in some massive stars near the main sequence (Venn et al. 2001), and we are now in the process of quantitatively constraining this mixing with age, mass, and rotation rate by analyzing boron-poor stars in clusters. |